adsabs/AstroCLIMB huggingface dataset:
Paper: The X–shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
Authors: Emanuele Paolo Farina, Jan-Torge Schindler, Fabian Walter, Eduardo Bañados, Frederick B. Davies, Roberto Decarli, Anna-Christina Eilers, Xiaohui Fan, Joseph F. Hennawi, Chiara Mazzucchelli, Romain A. Meyer, Benny Trakhtenbrot, Marta Volonteri, Feige Wang, Gábor Worseck, Jinyi Yang, Thales A. Gutcke, Bram P. Venemans, Sarah E. I. Bosman, Tiago Costa, Gisella De Rosa, Alyssa B. Drake, Masafusa Onoue
Figure caption: Black hole mass vs. FWHM of the Mg II line for the 28 quasars in our sample for which both the Mg II and C IV lines were successfully fitted (see Section 3.3). Pink triangles, green triangles, blue squares, and orange diamonds mark masses obtained with the Vestergaard & Peterson (2006), Coatman et al. (2017), Vestergaard & Osmer (2009), and Shen et al. (2011) estimators, respectively (see Table 4). Pale gray lines connect different mass estimates of the same object. The histograms on the right illustrate how the different recipes affect the mass distribution (the color scheme is the same as in the main panel). Horizontal dashed lines locate the corresponding averages. The average (median) masses of this subsample are 3.3×, 2.1×, 6.1×, and 2.2 × 109 M ⊙ (3.1×, 2.0×, 3.1×, and 2.0 × 109 M ⊙) if calculated with the Shen et al. (2011), Vestergaard & Osmer (2009), Vestergaard & Peterson (2006), and Coatman et al. (2017) estimators, respectively. The scatter plot on the bottom displays mass differences with respect to the Shen et al. (2011) estimator (see Section 4.2).
Paper: Discovery of a Radio-loud Narrow-line Seyfert 1 Galaxy at z = 0.9 Reddened with a Strong 2175 Å Bump
Authors: Yipeng Zhou, Lei Hao, Peng Jiang, Xiang Pan, Luming Sun, Chichuan Jin, Xuejie Dai, Wenjuan Liu, Tuo Ji, Zhenya Zheng, Xiangning Huang, Xiheng Shi, Yibo Wang, Yifei Xiong, Chenwei Yang
Figure caption: The dereddened spectra of the unusual quasars are compared with J1605+4743 and the averaged template in their Mg II(left panels), Hβ+O III (middle panels), and Hα emission lines (right panels). Similar to J1605+4743, the unusual quasars have weak Mg II emission lines, associated Mg II absorptions, and relatively narrow Balmer emission lines.
Paper: The X–shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
Authors: Emanuele Paolo Farina, Jan-Torge Schindler, Fabian Walter, Eduardo Bañados, Frederick B. Davies, Roberto Decarli, Anna-Christina Eilers, Xiaohui Fan, Joseph F. Hennawi, Chiara Mazzucchelli, Romain A. Meyer, Benny Trakhtenbrot, Marta Volonteri, Feige Wang, Gábor Worseck, Jinyi Yang, Thales A. Gutcke, Bram P. Venemans, Sarah E. I. Bosman, Tiago Costa, Gisella De Rosa, Alyssa B. Drake, Masafusa Onoue
Figure caption: Eddington ratio distribution for the bright (top), intermediate (middle), and faint (bottom) samples of z ≳ 5.7 quasars in this study. For comparison, the Eddington ratios of the luminosity-matched samples are also shown. The rectangles on the top of each panel mark the median values of the different distributions and show that high-redshift quasars have higher median accretion rates than the lower-redshift ones for all luminosity ranges. The color code is the same as in Figure 6.
Paper: The X–shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
Authors: Emanuele Paolo Farina, Jan-Torge Schindler, Fabian Walter, Eduardo Bañados, Frederick B. Davies, Roberto Decarli, Anna-Christina Eilers, Xiaohui Fan, Joseph F. Hennawi, Chiara Mazzucchelli, Romain A. Meyer, Benny Trakhtenbrot, Marta Volonteri, Feige Wang, Gábor Worseck, Jinyi Yang, Thales A. Gutcke, Bram P. Venemans, Sarah E. I. Bosman, Tiago Costa, Gisella De Rosa, Alyssa B. Drake, Masafusa Onoue
Figure caption: Logarithmic Eddington ratio distributions for the full sample of z ≳ 5.7 quasars (orange for our X–shooter sample and violet for other studies) and for the bolometric luminosity-matched sample described in Section 5 (black hatched histogram). The high- and low-redshift distributions have similar dispersions (∼0.3), but z ≳ 5.7 quasars have a median Eddington ratio (top red rectangle) that is higher than their lower-redshift counterparts (top black rectangle). For the sake of comparison, we also show the sample of 0.35 < z < 2.79 SDSS quasars as a pale gray histogram.
Paper: The X–shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
Authors: Emanuele Paolo Farina, Jan-Torge Schindler, Fabian Walter, Eduardo Bañados, Frederick B. Davies, Roberto Decarli, Anna-Christina Eilers, Xiaohui Fan, Joseph F. Hennawi, Chiara Mazzucchelli, Romain A. Meyer, Benny Trakhtenbrot, Marta Volonteri, Feige Wang, Gábor Worseck, Jinyi Yang, Thales A. Gutcke, Bram P. Venemans, Sarah E. I. Bosman, Tiago Costa, Gisella De Rosa, Alyssa B. Drake, Masafusa Onoue
Figure caption: Atlas of the Mg II emission for the 32 quasars in our sample for which the line was successfully fitted. Quasars are ordered by redshift, from low redshift on the top left to the highest redshift on the bottom right. In the top panel, we show the spectrum (in different shades of purple) and the corresponding 1–σ error for each object. The fits to the Mg II broad line and the iron pseudo-continuum are shown in pink and green dashed lines, respectively. The combined best fit of the continuum and the broad-line emission (see Section 3.3) is plotted as a solid yellow line. Residuals are displayed in gray in the bottom panel. In each panel, the spectrum is displayed in a ±14,000 km s−1 range around the expected position of the Mg II line at the systemic redshift (z sys).
Paper: The X–shooter/ALMA Sample of Quasars in the Epoch of Reionization. II. Black Hole Masses, Eddington Ratios, and the Formation of the First Quasars
Authors: Emanuele Paolo Farina, Jan-Torge Schindler, Fabian Walter, Eduardo Bañados, Frederick B. Davies, Roberto Decarli, Anna-Christina Eilers, Xiaohui Fan, Joseph F. Hennawi, Chiara Mazzucchelli, Romain A. Meyer, Benny Trakhtenbrot, Marta Volonteri, Feige Wang, Gábor Worseck, Jinyi Yang, Thales A. Gutcke, Bram P. Venemans, Sarah E. I. Bosman, Tiago Costa, Gisella De Rosa, Alyssa B. Drake, Masafusa Onoue
Figure caption: Same as Figure 2, but showing the C IV emission for the subsample of 34 quasars for which the line was successfully fitted. Each panel plots a region ±17,000 km s−1 around the systemic redshift reported in Table 1.
Paper: Inpainting Hydrodynamical Maps with Deep Learning
Authors: Faizan G. Mohammad, Francisco Villaescusa-Navarro, Shy Genel, Daniel Anglés-Alcázar, Mark Vogelsberger
Figure caption: Top panels: Power spectra measured from the ground-truth gas temperature maps averaged over 3000 maps in the test set (black thick line with shaded band), from the input maps masked using irregular-shaped masks (left panels) or regular-shaped masks (right panels) that cover 15% (blue shaded line) and 30% (red thick line) of the total area. Results, after the reconstruction is applied, are shown as blue dots with error bars for masks covering 15% and with red dots with error bars for those covering 30% of the area. Bottom panels: ratio between the power spectra measured from the reconstructed P out and ground-truth maps P ref are shown when masks cover 15% (blue line with shaded band) and 30% (red line with shaded band) of the area. All errors shown as shaded bands or error bars refer to the error on the mean of 3000 estimates.
Paper: Inpainting Hydrodynamical Maps with Deep Learning
Authors: Faizan G. Mohammad, Francisco Villaescusa-Navarro, Shy Genel, Daniel Anglés-Alcázar, Mark Vogelsberger
Figure caption: Mean difference between the probability density functions of the min-max scaled and log10-transformed temperature maps, estimated from the model output and the corresponding ground-truth map averaged over 3000 maps in the test set, in units of the standard error on the mean. Continuous lines show results when data are masked using irregular masks, while dashed lines correspond to the cases when regular-shaped masks are employed. Blue and red lines correspond to masks covering 15% and 30% of the total area, respectively. Horizontal shaded bands delimit 1σ and 2σ intervals. It is evident from this figure that the difference between the probability density functions of the reconstructed values and their ground-truth counterpart is (i) larger in the low-intensity regime, (ii) larger for regular masks compared to the irregular masks covering the same extent, and (iii) positively correlated with the extent of the masked regions.
Paper: Inpainting Hydrodynamical Maps with Deep Learning
Authors: Faizan G. Mohammad, Francisco Villaescusa-Navarro, Shy Genel, Daniel Anglés-Alcázar, Mark Vogelsberger
Figure caption: Distribution of the p-values of the Kolmogorov–Smirnov test performed on the 3000 maps that form the test set. Blue and red histograms show results for masks covering 15% and 30% of the total area, respectively. Top panel: results applying irregular masks. Bottom panel: results when regular-shaped masks are used. For irregular masks, the observed distribution of the K-S test p-values in the top panel supports the null hypothesis that the pixel values of the reconstructed and ground-truth maps are drawn from the same distribution. For regular masks, the distributions seen in the bottom panel indicate that the model fails to match the probability density function of the pixel values in the ground-truth temperature maps.
Paper: Inpainting Hydrodynamical Maps with Deep Learning
Authors: Faizan G. Mohammad, Francisco Villaescusa-Navarro, Shy Genel, Daniel Anglés-Alcázar, Mark Vogelsberger
Figure caption: Two-dimensional maps of six different auxiliary fields not used in the network training. From top to bottom row: SIMBA-based gas temperature map (T SIMBA), gas density (M gas), total matter density (M tot), gas pressure (P), electron number density (n  e ), and the magnesium-to-iron ratio (Mg/Fe). Column-wise from left to right: ground truth (﹩{\mathrm{log}}_{10}\left({{\boldsymbol{I}}}_{\mathrm{gt}}\right)﹩), model output (﹩{\mathrm{log}}_{10}\left({{\boldsymbol{I}}}_{\mathrm{out}}\right)﹩), and the difference between the model output and the ground-truth maps (﹩{\mathrm{log}}_{10}\left({{\boldsymbol{I}}}_{\mathrm{out}}/{{\boldsymbol{I}}}_{\mathrm{gt}}\right)﹩). For a fixed row, the left two columns share the same color coding shown in the color bars on the left, while the range of the color map in the rightmost column is adapted to highlight the differences between the model output and the ground-truth map. The color bars on the right show the color coding for the rightmost column.
Paper: Inpainting Hydrodynamical Maps with Deep Learning
Authors: Faizan G. Mohammad, Francisco Villaescusa-Navarro, Shy Genel, Daniel Anglés-Alcázar, Mark Vogelsberger
Figure caption: Temperature maps extracted from the CAMELS test set. Different columns display results applying masks of different types and extents. We show the log10 of the temperature maps for better visualization. Rows in order from top to bottom show the ground-truth maps ﹩{\mathrm{log}}_{10}{{\boldsymbol{I}}}_{\mathrm{gt}}﹩, prediction of the network ﹩{\mathrm{log}}_{10}{{\boldsymbol{I}}}_{\mathrm{out}}﹩, and the difference between the ground truth and the output maps ﹩{\mathrm{log}}_{10}\left({{\boldsymbol{I}}}_{\mathrm{out}}/{{\boldsymbol{I}}}_{\mathrm{gt}}\right)﹩. The contours show the area delimited by the masks. The different panels in the top two rows share the same color scale, while the color range in the bottom row is adapted to highlight the structures in the plot.
Paper: Inpainting Hydrodynamical Maps with Deep Learning
Authors: Faizan G. Mohammad, Francisco Villaescusa-Navarro, Shy Genel, Daniel Anglés-Alcázar, Mark Vogelsberger
Figure caption: Two cases from the test set where the comparison of the pixel values distributions using the Kolmogorov–Smirnov test results in two extreme p-values: very low in the left column and very high in the right column. In both cases, irregular masks that cover 15% of the data are applied. The top row shows the ground-truth maps while the bottom row shows the reconstructed ones. In all panels, dark contours represent the edges of the binary mask. The reconstruction performs poorly in the large contiguous masked patch highlighted by the white arrow in the left column, resulting in a low p-value. Such large continuous patches are absent in the right column, and the model returns a near-perfect reconstruction and a high p-value.
Paper: Quantifying the Evidence Against a Mass Gap between Black Holes and Neutron Stars
Authors: L. M. de Sá, A. Bernardo, R. R. A. Bachega, J. E. Horvath, L. S. Rocha, P. H. R. S. Moraes
Figure caption: Left: resulting likelihood ratio from Equation (3) for varying values of n, for the full gap candidate sample (solid line) and with V723 Mon and OB110463 removed (dashed line). Both curves show a typical draw that results in a peak closest to the mean preferred n over random draws. The likelihood ratio peaks at n = 7 for the full sample and at n = 4 with those two candidates removed. Note that the solid line is divided by a factor of 2.5 × 106 to fit the scale with the dashed line, which is nonetheless still significant. Right: the PDF and the CDF for models varying between n = 0 (dashed line, desert gap) and n = 16 (thin solid line). The central thick solid line shows the preferred distribution of a depleted gap with n = 7. Notice that there is a maximum allowed height for the plateau so that it does not extend beyond the BH peak.
Paper: Quantifying the Evidence Against a Mass Gap between Black Holes and Neutron Stars
Authors: L. M. de Sá, A. Bernardo, R. R. A. Bachega, J. E. Horvath, L. S. Rocha, P. H. R. S. Moraes
Figure caption: Left: the probability of the existence of a desert gap with an upper limit 5 M ⊙ as a function of its lower limit, for the mixed distribution from Section 2 on its own (dotted line), including all gap candidates (solid line) and all gap candidates but V723 Mon and OB110462 (dashed line). Right: the probability of each object falling in a gap with an upper limit 5 M ⊙ as a function of its lower limit. The objects are labeled as, from the most to the least massive: GW200115 (a), GW190924 (b), OB110462 (c), J02515658 (d), V723 Mon (e), GW200210 (f), GW190814 (g), GW170817 (h), J0952 (i), J2215 (j), GW190917 (k), GW190425 (l). Galactic sources are plotted with a dashed line, and extragalactic with a full line.
Paper: Quantifying the Evidence Against a Mass Gap between Black Holes and Neutron Stars
Authors: L. M. de Sá, A. Bernardo, R. R. A. Bachega, J. E. Horvath, L. S. Rocha, P. H. R. S. Moraes
Figure caption: Cumulative distribution functions (CDFs) for the original mixed mass distribution (dashed line) and the mixed distribution plus the new gap objects (solid line), with the gap range delimited by the two vertical dashed lines. The shaded regions represent the interval between the maximal and minimal draws for the original mixed distribution alone (lighter shade) and the one with the new objects (darker shade). While the variation of the CDF is minimal in the NS range of ≲1.8 M ⊙, it becomes significant in the gap range, especially in the 2–3 M ⊙ interval, as can be more clearly seen in the inset. A pronounced increase in the CDF is also seen in the BH range beyond the gap, as a result of a greater proportion of objects lying within the gap region. A quantitative evaluation of these differences is discussed in the text.
Paper: Quantifying the Evidence Against a Mass Gap between Black Holes and Neutron Stars
Authors: L. M. de Sá, A. Bernardo, R. R. A. Bachega, J. E. Horvath, L. S. Rocha, P. H. R. S. Moraes
Figure caption: Joint empirical distributions for compact object masses as the Gaussian mixtures of the fits for NSs from Rocha et al. (2021) and BHs from Özel et al. (2010), weighted by sample sizes (95 NSs and 16 BHs), with the putative gap region between 2 and 5 M ⊙ highlighted in a darker shade. Also shown in the gap between the BH and second NS peaks are the nominal masses and 1σ confidence intervals for the candidate gap objects from Table 1.
Paper: Quantifying the Evidence Against a Mass Gap between Black Holes and Neutron Stars
Authors: L. M. de Sá, A. Bernardo, R. R. A. Bachega, J. E. Horvath, L. S. Rocha, P. H. R. S. Moraes
Figure caption: Mass distributions for the 12 gap candidates considered in the preceding analysis (names in bold) and for eight additional candidates. For PSR J1311-3430, PSR J1748-2021B, and 1E 1740.7-2942 only the available mass ranges are shown, while for the other objects we show both nominal values, 1σ (inner bars) and 90% (outer bars) confidence intervals. We highlight the gap range in gray.
Paper: Quantifying the Evidence Against a Mass Gap between Black Holes and Neutron Stars
Authors: L. M. de Sá, A. Bernardo, R. R. A. Bachega, J. E. Horvath, L. S. Rocha, P. H. R. S. Moraes
Figure caption: Nominal values and 1σ credibility ranges for the 95 NS mass measurements from Rocha et al. (2021), distinguished by system type.
Paper: Quantifying the Evidence Against a Mass Gap between Black Holes and Neutron Stars
Authors: L. M. de Sá, A. Bernardo, R. R. A. Bachega, J. E. Horvath, L. S. Rocha, P. H. R. S. Moraes
Figure caption: Nominal values and 1σ credibility ranges for the 16 BH mass measurements from Özel et al. (2010).
Paper: Solar Polar Magnetic Fields: Comparing Full-disk and High-resolution Spectromagnetograph Data
Authors: Gordon J. D. Petrie
Figure caption: Polar synoptic maps for the south (two left columns) and north (two right columns) poles during 2006–2017. The concentric circles are lines of constant latitude, or constant r polar in Equation (4), in increments of 5° from the pole, which is marked by a plus symbol. The axes indicate the coordinates defined in Equation (4). These maps are based on SOLIS/VSM LOS magnetograms covering 35 day intervals centered on March 6/September 8 for the south/north pole. Note the supergranular organization of the flux into small, strong concentrations and the polarity reversal from lower to progressively higher latitudes.
Paper: Solar Polar Magnetic Fields: Comparing Full-disk and High-resolution Spectromagnetograph Data
Authors: Gordon J. D. Petrie
Figure caption: Polar synoptic maps for the north pole from SOT/SP observations, vector-derived (﹩{B}_{r}^{\mathrm{vec}}﹩, two left columns) and LOS-derived (﹩{B}_{r}^{\mathrm{LOS}}﹩, two right columns), taken over the 35 day interval centered on the optimal observing day, September 8, for the north pole. The concentric circles are lines of constant latitude, or constant r polar in Equation (4), in increments of 5° from the pole which is marked by a plus symbol. The axes indicate the coordinates defined in Equation (4).
Paper: Solar Polar Magnetic Fields: Comparing Full-disk and High-resolution Spectromagnetograph Data
Authors: Gordon J. D. Petrie
Figure caption: Polar synoptic maps for the south pole from SOT/SP observations, vector-derived (﹩{B}_{r}^{\mathrm{vec}}﹩, two left columns) and LOS-derived (﹩{B}_{r}^{\mathrm{LOS}}﹩, two right columns), taken over the 35 day interval centered on the optimal observing day, March 6, for the south pole. The concentric circles are lines of constant latitude, or constant r polar in Equation (4), in increments of 5° from the pole, which is marked by a plus symbol. The axes indicate the coordinates defined in Equation (4).
Paper: Solar Polar Magnetic Fields: Comparing Full-disk and High-resolution Spectromagnetograph Data
Authors: Gordon J. D. Petrie
Figure caption: Estimates of the total net radial magnetic flux through each polar region as functions of time from the VSM and SOT/SP, using observations from each year when good spatial coverage is available. The polar fields are assumed to extend from the poles to ±60°. See the text for details. Mean radial magnetic field strengths over this latitude range are indicated by the axis on the right.
Paper: Solar Polar Magnetic Fields: Comparing Full-disk and High-resolution Spectromagnetograph Data
Authors: Gordon J. D. Petrie
Figure caption: For the south pole, the mean signed field components from the SOLIS/VSM (﹩{B}_{r}^{\mathrm{LOS}}﹩) and from the Hinode/SOT/SP (the vector radial component ﹩{B}_{r}^{\mathrm{vec}},﹩ the horizontal components ﹩{B}_{t}^{\mathrm{vec}}﹩ and ﹩{B}_{p}^{\mathrm{vec}},﹩ and the LOS-based radial component ﹩{B}_{r}^{\mathrm{LOS}}﹩) are plotted as functions of angular distance r polar from the pole in degrees, as defined by Equation (4).
Paper: Solar Polar Magnetic Fields: Comparing Full-disk and High-resolution Spectromagnetograph Data
Authors: Gordon J. D. Petrie
Figure caption: For the north pole, the mean signed field components from the SOLIS/VSM (﹩{B}_{r}^{\mathrm{LOS}}﹩) and from the Hinode/SOT/SP (the vector radial component ﹩{B}_{r}^{\mathrm{vec}},﹩ the horizontal components ﹩{B}_{t}^{\mathrm{vec}}﹩ and ﹩{B}_{p}^{\mathrm{vec}},﹩ and the LOS-based radial component ﹩{B}_{r}^{\mathrm{LOS}}﹩) as functions of angular distance r polar from the pole in degrees, as defined in Equation (4).
Paper: Reaction of N+ Ion with H2, HD, and D2 at Low Temperatures: Experimental Study of the Pathway to Deuterated Nitrogen-containing Molecules in the Interstellar Medium
Authors: Radek Plašil, Štěpán Roučka, Artem Kovalenko, Thuy Dung Tran, Serhiy Rednyk, Petr Dohnal, Dmytro Shapko, Dieter Gerlich, Juraj Glosík
Figure caption: Arrhenius plot of the reaction rate coefficients ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDa}}﹩, ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDb}}﹩, ﹩{k}_{{{\rm{N}}}^{+}}^{{{\rm{D}}}_{2}}﹩ obtained in the present work in comparison with ﹩{k}_{{{\rm{N}}}^{+}}^{{\rm{p}}\text{-}{{\rm{H}}}_{2}}﹩ and ﹩{k}_{{{\rm{N}}}^{+}}^{{\rm{o}}\text{-}{{\rm{H}}}_{2}}﹩ derived from the data by Zymak et al. (2013). The corresponding rate coefficients obtained from the fitted global model (model C in Table 2) are indicated by the solid curves (only the model values of ﹩{k}_{{{\rm{N}}}^{+}}^{{\rm{o}}\text{-}{{\rm{H}}}_{2}}﹩ are indicated by a dotted line to differentiate them from the nearly identical ﹩{k}_{{{\rm{N}}}^{+}}^{\mathrm{HDa}}﹩ curve).
Paper: Solar Polar Magnetic Fields: Comparing Full-disk and High-resolution Spectromagnetograph Data
Authors: Gordon J. D. Petrie
Figure caption: The VSM and the SP vector- and LOS-derived south polar synoptic maps on a common scale for direct comparison, for the years of overlap between the VSM and SP data sets, from 2013 until 2017. The north polar data show similar agreement but were much weaker overall during this time.